As the analysis of the nebular spectrum in [1]} was mostly
qualitative, we aim to characterise the inner ejecta more quantitatively. In
particular, we determine the abundance and distribution of the central oxygen.
To this end we use our non-local thermodynamic equilibrium (NLTE) SN nebular
code, which is briefly described in Section . Before that, we
present a low resolution spectrum of SN 2010lp obtained at Gemini that had not
been analysed before. As the spectrum shows interstellar Na i D absorptions
from both the Galaxy and the host [1]}, it is very useful in order independently to determine the
reddening to SN 2010lp (Sect. ), which turns out to be smaller
than previously estimated. In Sect.  our possible solution for
the nebular spectrum of SN 2010lp is presented, and in Sect.  our
results and their implications are discussed. Sect.  concludes
the paper.
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